Table C.1
Quantities included in the current data release of the iEDGE.
| Database entry | Unit | Description |
|---|---|---|
| (1) | (2) | (3) |
| CALIFA_name | Name of the galaxy as indicated in the CALIFA extended DR3 | |
| Alias | Alternative name of the galaxy | |
| RA | deg | Right ascension of the galaxy centre |
| DEC | deg | Declination of the galaxy centre |
| Vlsr | km s−1 | LSR velocity of the galaxy, derived from the stellar redshift |
| zstar | Stellar redshift of the galaxy | |
| Distance | Mpc | Distance to the galaxy |
| Incl | deg | Galaxy inclination |
| PA | deg | Galaxy position angle |
| Re_as | arcsec | Galaxy effective radius |
| Type_med_EWHa | Å | Median Hα equivalent width |
| Type_Mstar | M⊙ | Stellar mass |
| Type_SFR | M⊙ yr−1 | Star formation rate derived using Balmer decrement |
| Type_sSFR | yr−1 | Specific star formation rate |
| Err_Type_Mstar | M⊙ | Uncertainty on the stellar mass |
| Err_Type_SFR | M⊙ yr−1 | Uncertainty on the star formation rate derived using Balmer decrement |
| Err_Type_sSFR | yr−1 | Uncertainty on the specific star formation rate |
| Type_Gas_Met | Gas-phase metallicity derived via the O3N2 method | |
| Type_alpha_co10 | M⊙ (K km s−1)−1 | CO(1-0)-to-H2 conversion factor derived following Bolatto et al. (2013) |
| Type_R21 | CO(2-1)/CO(1-0) flux ratio derived from the star formation rate surface density | |
| Observatory_Type_k2jypb | Jy beam−1 K−1 | Jy/beam per Kelvin |
| Observatory_Type_eta_mb | Main beam efficiency | |
| Observatory_Type_RMS | K | CO noise level (standard deviation of CO spectrum, σRMS) |
| Observatory_Type_Tpeak | K | Peak Tmb across the CO spectrum |
| Observatory_Type_SNR | Signal-to-noise ratio of the CO observation | |
| Observatory_Type_W50_mom2 | Full-width half maximum of the CO spectrum calculated via moment 2nd | |
| Observatory_Type_eps_obs | K km s−1 | Statistical error for the CO flux |
| Observatory_Type_Fco | Jy beam−1 km s−1 | CO flux |
| Observatory_Type_Lco | K km s−1 pc2 | CO luminosity |
| Observatory_Type_Mmol | M⊙ | Molecular gas mass |
| Observatory_Type_fmol | Molecular gas mass to stellar mass ratio | |
| Observatory_Type_SFE | yr−1 | Star formation efficiency |
| Final_Type_Observatory | Observatory of the CO measurement included in the consolidated sample | |
| Final_Type_SNR | Signal-to-noise ratio of the CO observation from the consolidated sample | |
| Final_Type_Mmol | M⊙ | Molecular gas mass from the consolidated sample |
| Final_Type_fmol | Molecular gas mass fraction from the consolidated sample | |
| Final_Type_SFE | yr−1 | Star formation efficiency from the consolidated sample |
| Observatory_Err_Type_Fco | Jy beam−1 km s−1 | Uncertainty on the CO flux |
| Observatory_Err_Type_Lco | K km s−1 pc2 | Uncertainty on the CO luminosity |
| Observatory_Err_Type_Mmol | M⊙ | Uncertainty on the molecular gas mass |
| Observatory_Err_Type_fmol | Uncertainty on the molecular gas mass to stellar mass ratio | |
| Observatory_Err_Type_SFE | yr−1 | Uncertainty on the star formation efficiency |
| Final_Err_Type_Mmol | M⊙ | Uncertainty on the molecular gas mass from the consolidated sample |
| Final_Err_Type_fmol | Uncertainty on the molecular gas fraction from the consolidated sample | |
| Final_Err_Type_SFE | yr−1 | Uncertainty on the star formation efficiency from the consolidated sample |
| Type_L12um_w3_7p5 | K km s−1 pc2 | 12 μm luminosity from WISE W3 at 7.5 arcsec resolution |
| Err_Type_L12um_w3_7p5 | K km s−1 pc2 | Uncertainty on the 12 μm luminosity from WISE W3 at 7.5 arcsec resolution |
| CARMA_conf | Array configuration of the CARMA observations | |
| Morphology | Galaxy morphology obtained from Hyperleda | |
Notes. Type considers global (Glob) and beam (Beam) quantities included in the database. Observatory indicates the facility from which the CO observation was performed (APEX, CARMA, or ACA). In the case a given source was not observed with the facility, the quantity assumes a NaN entry. Quantities measured from non-detected CO observation (with S/N<3) are included as upper limits. For the morphology, we simply separated the galaxies as spiral (S), elliptical (E), lenticular (S0), and irregular (I), without considering the sub-classes of spirals (except intermediate spirals, SABs; and barred spirals, SBs) and elliptical morphologies. Galaxies for which the morphology is not provided are indicated with ‘U’.
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